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The star CoRoT102781750 reveals a puzzle, showing a very complex and alteringvariation in different `CoRoT colours'. We established without doubt that morethan a single star was situated within the CoRoT mask. Using a search forperiodicity as a tool, our aim is to disentangle the composite light curve andidentify the type of sources behind the variability. Both flux and magnitudelight curves were used. Conversion was applied after a jump- andtrend-filtering algorithm. We applied different types of period-findingtechniques including MuFrAn and Period04. The amplitude and phase peculiaritiesobtained from the independent analysis of CoRoT r, g, and b colours andground-based follow-up photometric observations ruled out the possibility ofeither a background monoperiodic or a Blazhko type RR Lyrae star being in themask. The main target, an active star, shows at least two spotted areas thatreveal a $P_rot = 8.8$ hours $(f_0 = 2.735$ c d$^{-1})$ mean rotation period.The evolution of the active regions helped to derive a period change of $dP/dt= 1.6\cdot 10^{-6}$ (18 s over the run) and a differential rotation of $\alpha= \Delta\Omega/\Omega = 0.0074$. The $0\fm 015$ linear decrease and a local$0\fm 005$ increase in the dominant period's amplitude are interpreted as adecay of the old spotted region and an appearance of a new one, respectively. Astar that is detected only in the CoRoT b domain shows a $f_1 = 7.172$ cd$^{-1}$ pulsation connected to a $14\fd 83$ periodicity via an equidistanttriplet structure. The best explanation for our observation is a $\beta$ Cepstar with a corotating dust disk.

Periodicity search as a tool for disentangling the contaminated colour light curve of CoRoT 102781750